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Electron acceleration by Alfven waves in the
magnetosphere
Peter Damiano and Jay Johnson Princeton Plasma Physics Laboratory
(image courtesy of NASA)
PPPL Theory Research and Review Seminar - Jan 23, 2015
Magnetosphere-Ionosphere Coupling
ou#low
Magnetosphere-Ionosphere Coupling
ou#lowMagnetospheric configuration changes drive Field Aligned Currents (FAC)
FAC
Magnetosphere-Ionosphere Coupling
ou#lowFACs carry electron flux into ionosphere
FAC
Electron flux interacts with atmospheric gases to produce aurora
Magnetosphere-Ionosphere Coupling
ou#lowPoynting and Electron flux also drive outflow of heavy ions
FAC
Which alters the magnetospheric configuration
• Monoenerge+c Aurora are associated with– quasi-‐sta+c global Field Aligned Currents– Low frequency Alfven waves
• Broadband Aurora are associated with– kine+c scale Alfven waves (λ⊥~c/ωpe, ρs or ρi) – and can drive substan+al ou#low
• Diffuse Aurora– EMIC and whistler waves (radia+on belts).
Auroral Morphology
Fundamental Ques+ons: • How and where are e-‐ accelerated to carry FACs?• How does wave energy reach dispersive scales?• How do auroral arcs form? • What is feedback on global system?
Chaston et al., 2008
R(*E(* 1%)(&&*)(S * 1) )*: &*8
+,-./#"0."(
91: ;')$4(# ??
()*+,
S"%-* 1)%)*'MC+L(#)(A TN
:%L( &*8(M!&JLU+*'N
QQ 8E
-" -.
*/-012
32*04(-"
35-/67245*QQ 8E
*)"A
(
35*/-012
89V&(')#$+ V+(#K5 B&"W%) C$+$-2/(#(
3%)*
-.%) C$+$-2/(#(ME:XE
Mono-energetic Aurora and low frequency Alfven waves
Field Line Resonance
xmxr
xt
xr xt xmx
VA(x)
ξx
Field Line Resonances (standing Alfven waves) and auroral arcs
FLRs can be generated by mode conversion from fast mode
magnetopause boundary
fast mode
Long extended arc in azimuthal direc+on (out of page)
(Samson et al., 2003)
(mHz frequency wave)
(Samson et al., 2003)
Longitude 340o330o
La+tud
e
63o
66o
What generates E|| in Alfven waves?
• Dispersive wave effects -‐ (e.g. Wei et al., 1994; Streltsov and Lotko 1996; Bhaaacharjee, et al. 1999; Wright et al., 2002).
• Anomalous resis+vity (Lysak and Dum, 1983; Lotko et al., 1998).
• Mirror force effects (Rankin et al., 1999).
Ques+ons: Can we generate sufficient E|| due to mirror force effects in a self-‐consistent kine+c simula+on to accelerate electrons to keV energies? What are signatures of accelera+on?
Need E|| to accelerate trapped electrons to carry j||
Guiding center equations
Faraday’s Law
Momentum equation
Cold Plasma MHD equations
(Damiano et al., Phys. Plasmas, 14, 062904, 2007)
Perpendicular Ohm’s law
E? = �u�Bo
me
dv||dt
= �eE|| � µmr||Bo
h||dx||dt
= v||
�b��t
=�1
h||h�
�
�x||(h�E�)�
�
�x�(h||E||)
�
µo�o⇥u�⇥t
=Bo
h||h�
⇥
⇥x||(h�b�)
�
coupling via E|| (Gen. Ohm’s Law including moments of e- distribution function)
Particle/field interpolation done using standard PIC techniques.
2D hybrid MHD-kinetic electron model
x||x
x
mirror force term
Parallel (L=10)
iono
sphe
re
iono
sphe
re
Equator
Ionosphere
L=10
L=9.4
Perpendicular
Half-Gaussian results in only region of upward FAC
Ionospheric boundary at altitude of 1 Re
Initial Perturbation
Feedback in hybrid model • Perpendicular dispersion (S⊥=-‐E||bφ)• Cross scale coupling
x||x
x
Plot northern hemisphere in dipolar coordinates
Field Aligned Current Density
Larger Te -‐> increased mirror force trapping -‐> remaining current carriers must be accelerated to higher velocity.
0.00 0.05 0.10 0.15 0.20 0.25time (TA)
0.0
0.4
0.8
1.2
1.6
2.0
2.4
2.8
3.2
3.6
4.0
elec
tron
ener
gy (k
eV)
0.0
0.2
0.4
0.6
0.8
1.0
Mirror force effects can accelerate electrons to keV energies
Te=200 eV
0.00 0.05 0.10 0.15 0.20 0.25time (seconds)
0.0
0.4
0.8
1.2
1.6
2.0
2.4
2.8
3.2
3.6
4.0
elec
tron
ener
gy (k
eV)
0.0
0.2
0.4
0.6
0.8
1.0
Te=keV
Electron acceleration is a large sink of wave energy
mono-energetic beam
Significant energy dissipation
Un-driven resonance would completely damp in < 2 TA -> same magnitude as Ohmic dissipation in ionospheric currents.
0 500 1000 1500 2000 2500e Δ Φ (eV)
-0.3
-0.2
-0.1
0
j 1 (µ
A/m
2 )
t=0.15 TA
0 500 1000 1500 2000 2500e Δ Φ (eV)
-0.3
-0.2
-0.1
0
j 1 (µ
A/m
2 )
t=0.2 TAt=0.25 TA
0.00 0.05 0.10 0.15 0.20 0.250.00.40.81.21.62.02.42.83.23.64.0
elec
tron
ener
gy (k
eV)
0.0
0.2
0.4
0.6
0.8
1.0
(a)
0.00 0.05 0.10 0.15 0.20 0.25time (TA)
0.0
0.2
0.4
0.6
0.8
1.0
Wav
e en
ergy
(nor
mal
ized
)
MHDTe=1000 eV
(b)
Te=keV
Broadband Aurora and Dispersive Alfven waves
Broadband e-‐ precipita+on correlated with Alfvenic Poyn+ng flux.
(Wing et al., 2013) (Keiling et al., 2003)
Broadband electron energy flux Downward Alfvenic PoynIng flux
Poyn+ng flux associated with ~Hz frequency dispersive Alfven waves (λ|| ~ RE, λ⊥ ~ λe, ρs, ρi).
Sun
Mo+va+on -‐ Understanding forma+on of Broadband Aurora
Broadband aurora increase rapidly at onset (e.g. Wing et al., 2013).
Is dispersive scale structuring imposed at onset site or after?
Mo+va+on -‐ Substorm onset and Broadand Aurora
Understanding transit time of waves to ionosphere is important to help connect optical signatures to driving mechanism.
Wave observations (e.g. Lessard et al., 2006, Chi et al., 2009) used to evaluate onset timing and location.
Breaking of fast flows is one observed source of KAWs
(Lessard et al., 2006, 2011)
Characteristics of wave-particle interactions depend on location
Fermi accelera+on Par+cle trapping
(Kletzing et al., 1994)
(Waa
and
Rankin, 2010)
IAW regime
Path along field line is a highly variable plasma environment
Alfven wave KAW regime
vth < VA
vth > VA
• Loca+on/mechanism for accelera+on not clearly established.• Means by which energy reaches dispersive scales not known.• Studies to date, informa+ve but are mostly 1D or local. • Limited explora+on of ρi effects (Ti/Te ~ 7 in plasma sheet).
Faraday’s Law
Modified Momentum equation
Modified Perpendicular Ohm’s law
where
h||dx||dt
= v||
Hybrid gyrofluid-kinetic electron model in curvilinear coordinates
Cold Plasma MHD equations Guiding center equations
@b�
@t
=�1
h||h?
@
@x||(h?E?)�
@
@x?(h||E||)
�
me
dv||dt
= �eE|| � µmr||Bo
ũ� = (1� 1.25⇢2ir2?)u�
E? = �Bo(ũ� � ⇢2i
r2?ũ�)
x||x
x
coupling via E|| (Gen. Ohm’s Law including moments of e- distribution function)
(Damiano et al., Phys. Plasmas, 14, 062904, 2007, Cheng and Johnson, 1999, Damiano et al., 2015)
µ
o
⇢
o
@ũ
�
@t
=B
o
h||h�
@
@x||(h
�
b
�
)
�
perpendicular E⊥ profile at equator
λ⊥~ 0.1 RE
Identical pulses propagate to each field-aligned boundary (at 1 RE altitude above Earth surface).
Field line of maximum upward current
Kine+c Alfven wave pulse – ini+al perturba+on example
Initialize KAW perturbation in the plasma sheet
9.4 9.6 9.8 10
ro (RE)
-10
-5
0
5
10
E⊥ (
mV
/m)
(b)
Two simulation cases: 1) Ti=0, Te=100 eV2) Ti=1 keV, Te=100 eV
k?k||
⇠ 10
k?k||
⇠ 10� 100 (Chaston et al., 2014)
Increased phase speed, but reduced coupling
k?⇢i ⇠ 1
k?⇢i ⇠ 2
E||E?
=�k||k?⇢2s(1 + k2?⇢
2i )
Also evident in 2 fluid analysis(e.g. Chaston et al., 2003)
Hot Ion
Cold Ion
0 1 2 3 4 5 6 7 8l|| (RE)
-1
-0.5
0
j || / |
j ||m
ax (T
i=0)
|Ti=0, Te=100 eV
(a)Ti=1 keV, Te=100 eV
λ⊥eq=0.1 RE
0 1 2 3 4 5 6 7 8l|| (RE)
-1
-0.5
0
j || / |
j ||m
ax (T
i=0)
|
(b)
λ⊥eq=0.05 RE
t=8 s
! = k||VA
r1 + k2?⇢
2i (1 +
TeTi
)In plasma sheet, Te/Ti ~ 1/7
(Baumjohann et al., 1987)
(e.g. Tatsuno et al., 2009)
!
k||= VA ⇠ 0.2⇥ 107m/s
Electron distribu+on func+on evolu+on
0 1 2 3 4 5 6 7 8 9 10l|| (RE)
0
0.5
1
1.5
2
2.5
3
V A (×
107
m/s
)
0 2 4 6 8 10l|| (RE)
-0.08
-0.06
-0.04
-0.02
0
j || (µ
A/m
2 )
Ti=0, t=30 sTi=1 keV, t=22 s
(a)
0 0.5 1 1.5|v⊥| (10
7 m/s)
-1.5
-1
-0.5
0
0.5
1
1.5
v || (1
07 m
/s)
t=30 s
(b)
0 0.5 1 1.5|v⊥| (10
7 m/s)
-1.5
-1
-0.5
0
0.5
1
1.5t=22 s
(c)
Parallel elongation in distribution function is qualitatively consistent with observations (e.g. Wygant, 2000) and simulations (Watt and Rankin, 2009)
Superposition at same l||=5 RE, but different times
More perpendicular dispersion for increased Ti
0 2 4 6 8 10l|| (RE)
-0.08
-0.06
-0.04
-0.02
0
j || (µA/m
2 )
Ti=0, t=30 sTi=1 keV, t=22 s
(a)
0.1 0.102 0.104 0.106x⊥
-0.08-0.06-0.04-0.02
00.020.040.060.08
j || (µA/m
2 )
l||=5 RE
(b)
Ionospheric Evolu+on
0 5 10 15 20 25 30 35 40time (seconds)
-0.8
-0.6
-0.4
-0.2
0
j || (µA/m
2 )
Ti=0Ti=keV
(a)
0 0.5 1 1.5 2Energy (keV)
1
101
102
103
104
Ne
(b)
t=37 st=30 s
Broadband energization
ρi effects limit current and electron energiza+on all along field line
• Mirror force effects in global scale Alfven waves self-‐consistently produce sufficient ΔΦ|| to accelerate electrons to keV energies (consistent with observa+ons).
• Electron accelera+on is a significant sink of wave energy.• Consistent with observa+ons, electron accelera+on in dispersive
scale Alfven waves is broadband in nature
• ρi effects significantly shorten transit +me of Alfven wave to the ionosphere but reduce the ability of the wave to energize electrons.
• E|| effects (on all scales) cause a perpendicular dispersion of wave energy.
Summary
• Mirror force effects in global scale Alfven waves self-‐consistently produce sufficient ΔΦ|| to accelerate electrons to keV energies (consistent with observa+ons).
• Electron accelera+on is a significant sink of wave energy.• Consistent with observa+ons, electron accelera+on in dispersive
scale Alfven waves is broadband in nature
• ρi effects significantly shorten transit +me of Alfven wave to the ionosphere but reduce the ability of the wave to energize electrons.
• E|| effects (on all scales) cause a perpendicular dispersion of wave energy.
Summary
Fundamental Ques+ons: • How and where are e-‐ accelerated to carry FACs?• How does wave energy reach dispersive scales? • How do auroral arcs form?• What is feedback on global system?
• Broadband aurora -‐ parameter study (k⊥, k||, E⊥,Ti, Te).• ρi effects on Field Line Resonances -‐ affects E|| profile (Streltsov et al.,
1998) -‐ observed (Chaston et al., 2013).• Fast mode dynamics and mode conversion (relevant to both Field Line
Resonances and broadband aurora) -‐ stretched tail topologies (MAG2D)
• Ionospheric coupling -‐ (ionospheric dissipa+on, return currents, mul+-‐period simula+ons -‐> auroral arc forma+on, evolu+on)
• Cross-‐scale coupling of wave energy [phase mixing, wave-‐wave coupling (nonlinear MHD/3D), wave par+cle interac+ons, ionospheric feedback].
• Nonlinear sta+onary iner+al Alfven waves (nonlinear MHD).• More systema+c comparison with satellite observa+ons (e.g FAST, Polar,
Themis).
• More realis+c driving.
Future directions
Extra Slides
(plus auxiliary Poisson’s equaIon to enforce quasi-‐neutrality)
Moments of electron distribuIon funcIon determined from kineIc electrons using ParIcle-‐In-‐Cell (PIC) techniques.
(Damiano et al., Phys. Plasmas, 14, 062904, 2007)
KAW
Mirror force terms
Generalized Ohm’s Law
@
@x?
h
�
h||h?
✓@(h||E||)
@x?
◆��
h||E||
�
2e
=@
@x?
✓h
�
h||h?
@
@x||(h?E?)
◆
+ eµo
@
@x||
Zv
2||fed
3v
+ µo
e
m
e
@B
o
@x||
Zµ
m
f
e
d
3v
� 2µo
e
m
e
@B
o
@x||
Zm
e
v
2||
2Bo
f
e
d
3v